Qastrocam-g2 is a fork of the Qastrocam project, Webcam capture software for astronomy. This fork adds support for RGB24 (luminance only) and YUYV. It has better generic V4L support (lx mode and resizing). Settings backup has been added. There is better parallel and serial lx mode support. There are a number of other changes and additions.
WCSLIB is a C library, supplied with a full set of Fortran wrappers, which implements the "World Coordinate System" (WCS) standard in FITS (Flexible Image Transport System). It also includes a PGPLOT-based routine, PGSBOX, for drawing general curvilinear coordinate graticules, and a number of utility programs. The FITS "World Coordinate System" (WCS) convention defines keywords and usage which provide descriptions of astronomical coordinate systems in a FITS image header.
SAOTrace is a suite of software designed to simulate the as-built performance of grazing-angle X-ray optics using the ray-tracing approach. It is derived from portions of the NASA OSAC (Optical Surface Analysis Code) software suite. It can model nested conical as well as flat optical designs, and includes the ability to model arbitrary support structures and baffles. It can model non-ideal multi-layer reflective coatings as well as scattering from the optical surfaces.
PAPFIP (Python And PGPLOT-based FITS Image Plotter) is a FITS image plotter based on the Python bindings to the pgplot graphics library. It is intended as a non-interactive (command line or script-driven) astronomical image plotter intended for the automated or repeated production of finalized publication-quality Postscipt files, rather than a method of inspecting or visualizing the data.
Remote Telescope System (RTS2) is an integrated system for remote observatory control. It is designed to keep an observatory running, protect it from elements, take images, ensure that pointing is good, react to TOOs, keep track of what was done, send you data, and help you to do science. It picks targets from a database table, stores image meta-data in a database, processes images, and stores WCS coordinates in the database. An abstract device layer enables control of all possible combinations of mounts, CCDs, photometers, and roof and cupola controllers.
ccurve_create.tcl is a TCL script (plus associated csh scripts) that makes it is possible to calculate cooling curves (plasma emissivities, in units of erg cm^3 s^-1) as a function of plasma temperature using the hot plasma codes available in the XSPEC spectral fitting program. Element-or-line-specific cooling functions can also be created. These can be used in hydrodynamical simulations to assess the total cooling rate, calculate the luminosity in a specific wavelength/energy range, or more generally to calculate X-ray or UV line diagnostics.